%0 Journal Article
%A Rodríguez Muñoz, L.
%A Rodighiero, G.
%A Mancini, C.
%A Pérez González, Pablo Guillermo
%A Rawle, T.D.
%A Egami, E.
%A Mercurio, A.
%A Rosati, P.
%A Puglisi, A.
%A Franceschini, A.
%A Balestra, I.
%A Baronchelli, I.
%A Biviano, A.
%A Ebeling, H.
%A Edge, A,C,
%A Enia, A.F.M.
%A Grillo, C.
%A Haines, C.P.
%A Iani, E.
%A Jones, T.
%A Nonino, M.
%A Valtchanov, I.
%A Vulcani, B.
%A Zemcov, M.
%T Quantifying the suppression of the (un)-obscured star formation in galaxy cluster cores at 0.2  </~ z </~ 0.9
%D 2019
%@ 0035-8711
%U https://hdl.handle.net/20.500.14352/13587
%X We quantify the star formation (SF) in the inner cores (R/R_(200) ≤0.3) of 24 massive galaxy clusters at 0.2  </~ z </~ 0.9 observed by the Herschel Lensing Survey and the Cluster Lensing and Supernova survey with Hubble. These programmes, covering the rest-frame ultraviolet to far-infrared regimes, allow us to accurately characterize stellar mass-limited (M∗ > 10^(10) Mꙩ) samples of star-forming cluster members (not)-detected in the mid- and/or far-infrared. We release the catalogues with the photometry, photometric redshifts, and physical properties of these samples. We also quantify the SF displayed by comparable field samples from the Cosmic Assembly Near-infrared Deep Extragalactic Legacy Survey. We find that in intermediatez cluster cores, the SF activity is suppressed with respect the field in terms of both the fraction (F) of star-forming galaxies (SFGs) and the rate at which they form stars (SFR and sSFR = SFR/M∗). On average, the F of SFGs is a factor ∼2 smaller in cluster cores than in the field. Furthermore, SFGs present average SFR and sSFR typically ∼0.3 dex smaller in the clusters than in the field along the whole redshift range probed. Our results favour long time-scale quenching physical processes as the main driver of SF suppression in the inner cores of clusters since z ∼0.9, with shorter time-scale processes being very likely responsible for a fraction of the missing SFG population.
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